  We present a detailed analysis of the progenitor and its local environment
for the recently discovered type II supernova (SN) 2024ggi at a distance of
about 6.7~Mpc, by utilizing the pre-explosion images from the Hubble Space
Telescope (HST) and \textit{Spitzer} Space Telescope. The progenitor is
identified as a red, bright variable star, with absolute $F814W$-band
magnitudes being $-$6.2 mag in 1995 to $-$7.2 mag in 2003, respectively,
consistent with that of a normal red supergiant (RSG) star. Combining with the
historical mid-infrared light curves, a pulsational period of about 379~days
can be inferred for the progenitor star. Fitting its spectral energy
distribution with stellar spectral models yields the stellar parameters of
temperature, radius and bolometric luminosity as $T_*=3290_{-27}^{+19}$~K,
$R_*=887_{-51}^{+60}$~R$_{\odot}$, and
log($L$/L$_{\odot}$)$=4.92_{-0.04}^{+0.05}$, respectively. The above parameters
indicate that the progenitor of SN 2024ggi is consistent with the stellar
evolutionary track of a solar-metallicity massive star with an initial mass of
$13_{-1}^{+1}$~M$_{\odot}$. Moreover, our analysis indicates a relatively low
mass loss rate (i.e., $< 3\times10^{-6}$~M$_{\odot}$~yr$^{-1}$) for the
progenitor compared to that inferred from the flashed spectra and X-ray
detection (i.e., $10^{-2}$$-$$ 10$$^{-5}$~M$_{\odot}$~yr$^{-1}$), implying a
significant enhancement in mass loss within a few years prior to the explosion.
