We show that the cool gas masses of galactic discs reach a steady state that lasts many Gyr after their last major merger in cosmological hydrodynamic simulations. The mass of disc gas, M$_{rm gas}$, depends upon a galaxy halos spin and virial mass,
but not upon stellar feedback. Halos with low spin have high star formation efficiency and lower disc gas mass. Similarly, lower stellar feedback leads to more star formation so the gas mass ends up nearly the same irregardless of stellar feedback strength. Even considering spin, the M$_{rm gas}$ relation with halo mass, M$_{200}$ only shows a factor of 3 scatter. The M$_{rm gas}$--M$_{200}$ relation show a break at M$_{200}$=$2times10^{11}$ M$_odot$ that corresponds to an observed break in the M$_{rm gas}$--M$_star$ relation. The constant disc mass stems from a shared halo gas density profile in all the simulated galaxies. In their outer regions, the profiles are isothermal. Where the profile rises above $n=10^{-3}$ cm$^{-3}$, the gas readily cools and the profile steepens. Inside the disc, rotation supports gas with a flatter density profile except where supernova explosions disrupt the disc. Energy injection from stellar feedback also provides pressure support to the halo gas to prevent runaway cooling flows. The resulting constant gas mass makes simpler models for galaxy formation possible, either using a bathtub model for star formation rates or when modeling chemical evolution.
