We present the confirmation of the eccentric warm giant planet TOI-201 b, first identified as a candidate in \textit{TESS} photometry (Sectors 1-8, 10-13, and 27-28) and confirmed using ground-based photometry from NGTS and radial velocities from FEROS, HARPS, CORALIE, and \textsc{Minerva}-Australis. TOI-201 b orbits a young (\(\mathrm{0.87^{+0.46}_{-0.49} \, Gyr}\)) and bright(V=9.07 mag) F-type star with a \(\mathrm{52.9781 \, d}\) period. The planet has a mass of \(\mathrm{0.42^{+0.05}_{-0.03}\, M_J}\), a radius of \(\mathrm{1.008^{+0.012}_{-0.015}\, R_J}\), and an orbital eccentricity of \(0.28^{+0.06}_{-0.09}\); it appears to still be undergoing fairly rapid cooling, as expected given the youth of the host star. The star also shows long-term variability in both the radial velocities and several activity indicators, which we attribute to stellar activity. The discovery and characterization of warm giant planets such as TOI-201 b is important for constraining formation and evolution theories for giant planets.