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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 andradial velocities from FEROS, HARPS, CORALIE, and \textsc{Minerva}-Australis.TOI-201 b orbits a young ($\mathrm{0.87^{+0.46}_{-0.49} \, Gyr}$) andbright(V=9.07 mag) F-type star with a $\mathrm{52.9781 \, d}$ period. Theplanet 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-termvariability in both the radial velocities and several activity indicators,which we attribute to stellar activity. The discovery and characterization ofwarm giant planets such as TOI-201 b is important for constraining formationand evolution theories for giant planets.

A transiting warm giant planet around the young active star TOI-201