We present optical and near-IR imaging and spectroscopy of SGAS J 105039.6+001730, a strongly lensed galaxy at z = 3.6252 magnified by >30x, and derive its physical properties. We measure a stellar mass of log(M sub(*)/M sub(middot in circle)) = 9.5 + or - 0.35, star formation rates from OII 2.2.3727 and H beta of 55 + or - 25 and 84 + or - 24 M sub(middot in circle) yr super(-1), respectively, an electron density of n sub(e) < or =, slant 10 super(3) cm super(-2), an electron temperature of T sub(e) < or =, slant 14,000 K, and a metallicity of 12 + log(O/H) = 8.3 + or - 0.1. The strong C III lambdalambda1907,1909 emission and abundance ratios of C, N, O, and Si are consistent with well-studied starbursts at z ~ 0 with similar metallicities. Strong P Cygni lines and He II lambda1640 emission indicate a significant population of Wolf-Rayet stars, but synthetic spectra of individual populations of young, hot stars do not reproduce the observed integrated P Cygni absorption features. The rest-frame UV spectral features are indicative of a young starburst with high ionization, implying either (1) an ionization parameter significantly higher than suggested by rest-frame optical nebular lines, or (2) differences in one or both of the initial mass function and the properties of ionizing spectra of massive stars. We argue that the observed features are likely the result of a superposition of star forming regions with different physical properties. These results demonstrate the complexity of star formation on scales smaller than individual galaxies, and highlight the importance of systematic effects that result from smearing together the signatures of individual star forming regions within galaxies.