A simple cosmological model with only six parameters (matter density, Omega sub(m)h super(2), baryon density, Omega sub(b)h super(2), Hubble constant, H sub(0), amplitude of fluctuations, sigma sub(8), optical depth, tau , and a slope for the scalar perturbation spectrum, n sub(s)) fits not only the 3 year WMAP temperature and polarization data, but also small-scale CMB data, light element abundances, large-scale structure observations, and the supernova luminosity/distance relationship. Using WMAP data, only, the best-fit values for cosmological parameters for the power-law flat Lambda cold dark matter ( Lambda CDM) model are ( Omega sub(m)h super(2), Omega sub(b)h super(2),h,n sub(s), tau , sigma sub(8)) = (0.1277 super(+0.0080)-0.0079,0.02229 plus or minus 0.00073,0.732 super(+0.031)-0.032,0.958 plus or minus 0.016,0.089 plus or minus 0.030,0.761 super(+0.049)-0.048). The 3 year data dramatically shrink the allowed volume in mis six-dimensional parameter space. Assuming that the primordial fluctuations are adiabatic with a power-law spectrum, the WMAP data alone require dark matter and favor a spectral index that is significantly less than the Harrison-Zel'dovich-Peebles scale-invariant spectrum (n sub(s) = 1, r = 0). Adding additional data sets improves the constraints on these components and the spectral slope. For power-law models, WMAP data alone puts an improved upper limit on the tensor-to-scalar ratio, r sub(0.002) < 0.65 (95% CL) and the combination of WMAP and the lensing-normalized SDSS galaxy survey implies r sub(0.002) < 0.30 (95% CL). Models that suppress large-scale power through a running spectral index or a large-scale cutoff in the power spectrum are a better fit to the WMAP and small-scale CMB data than the power-law Lambda CDM model; however, the improvement in the fit to the WMAP data is only Delta chi super(2) = 3 for 1 extra degree of freedom. Models with a running-spectral index are consistent with a higher amplitude of gravity waves. In a flat universe, the combination of WMAP and the Supernova Legacy Survey (SNLS) data yields a significant constraint on the equation of state of the dark energy, w = -0.967 super(+0.073)-0.072. If we assume w = -1, then the deviations from the critical density, Omega sub(K) are small: the combination of WMAP and the SNLS data implies Omega sub(k) = -0.011 plus or minus 0.012. The combination of WMAP 3 year data plus the HST Key Project constraint on H sub(0) implies Omega sub(k) = -0.014 plus or minus 0.017 and Omega sub( Lambda ) = 0.716 plus or minus 0.055. Even if we do not include the prior that the universe is flat, by combining WMAP, large-scale structure, and supernova data, we can still put a strong constraint on the dark energy equation of state, w = -1.08 plus or minus 0.12. For a flat universe, the combination of WMAP and other astronomical data yield a constraint on the sum of the neutrino masses, capital sigma m sub( upsilon ) < 0.66 eV (95%CL). Consistent with the predictions of simple inflationary theories, we detect no significant deviations from Gaussianity in the CMB maps using Minkowski functionals, the bispectrum, trispectrum, and a new statistic designed to detect large-scale anisotropies in the fluctuations.