  AU Mic is a young, active star whose transiting planet was recently detected.
We report our analysis of its TESS data, where we modeled the BY Draconis type
quasi-periodic rotational modulation by starspots simultaneously to the flaring
activity and planetary transits. We measured a flare occurrence rate of 6.35
flares per day for flares with amplitudes in the range of $0.06\% < f_{\rm max}
< 1.5\%$ of the star flux. We employed a Bayesian MCMC analysis to model the
five transits of AU Mic b, improving the constraints on the planetary
parameters. The planet radius of $4.07\pm0.17$~R$_{\oplus}$ and a mean density
of $1.4\pm0.4$~g~cm$^{-3}$ confirms that it is a Neptune-size moderately
inflated planet. While a single feature possibly due to a second planet was
previously reported in the former TESS data, we report the detection of two
additional transit-like events in the new TESS observations of July 2020. This
represents substantial evidence for a second planet (AU Mic c) in the system.
We analyzed its three transits and obtained an orbital period of
$18.859019\pm0.000016$~d and a planetary radius of $3.24\pm0.16$~R$_{\oplus}$,
which defines it as a warm Neptune-size planet with an expected mass in the
range of 2.2~M$_{\oplus}$~$< M_{\rm c} < $25.0~M$_{\oplus}$. The two planets in
the system are in near 9:4 mean-motion resonance. We show that this
configuration is dynamically stable and should produce transit-timing
variations (TTV). Our non-detection of significant TTV in AU Mic b suggests an
upper limit for the mass of AU Mic c of $<7$~M$_{\oplus}$, indicating that this
planet is also likely to be inflated. As a young multi-planet system with at
least two transiting planets, AU Mic becomes a key system for the study of
atmospheres of infant planets and of planet-planet and planet-disk dynamics at
the early stages of planetary evolution.
