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We investigate the connection between the HI~content, SFR and environment ofgalaxies using a hydrodynamic simulation that incorporates scaling relationsfor galactic wind and a heuristic halo mass-based quenching prescription. Werun two zoom-in simulations of galaxy groups with $M_{halo}>10^{13}M_\odot$ atz=0, selected to have quiet merger histories. We track galaxies as they becomesatellites, and compute the delay time $\tau_{d}$ during which the satellitesare similar to central galaxies at a given stellar mass, and a fading time$\tau_{f}$ during which satellites go from gas-rich and star-forming togas-poor and quiescent. We find $0.7< \tau_{d}< 3$ Gyr at $z=0$, and dependsinversely on the satellite halo mass at infall. At z ~ 1 we find ~$0.3<\tau_{d} < 2$ Gyr, broadly consistent with a positive correlation with theHubble time. For a given halo mass, lower stellar mass galaxies at infall timehave higher $\tau_{d}$. We generally find $\tau_{f}\ll \tau_{d}$, rangingbetween ~ 150 Myr at z~0 and ~ 80 Myr at z ~ 1 based on linear interpolation,with some uncertainty because they are smaller than our simulation outputfrequency ($200-300$ Myr). $\tau_{f}$ has no obvious dependency on infall halomass. Both timescales show little difference between HI depletion and SFquenching, indicating that using up the gas reservoir by star formation withoutrefilling is the main mechanism to transform satellite galaxies at these halomasses. At a given physical distance from the center of the main halo ofinterest, higher redshift galaxies have on average higher cold gas content, butthe ratio of gas (HI or H$_2$) to star formation rate is similar, indicatingthat star formation is consistently fed through reservoirs of HI then H$_2$.For a given amount of HI, galaxies have shorter consumption times in moremassive halo structures.

Timescales for Hi consumption and SFR depletion of satellite galaxies in groups