Stars are formed in galaxies from the collapse of gas clouds composed mostly of hydrogen. It has been previously shown that the amount of gas in a galaxy depends on its shape and structure (its morphology), and that spiral galaxies tend to host more gas. Measuring gas content is somewhat difficult to do, so it would be beneficial to use easy-to-measure quantities to estimate gas content in galaxies. Our gas measurements are taken from archival data, yielding a sample of 230 galaxies with molecular hydrogen (H2) measurements and 4,094 with atomic hydrogen (HI) measurements. We examine the correlations between HI and H2 gas content and different structural parameters that measure the distribution of mass within the galaxies. We find that gas content is correlated most strongly with the density of stars in the inner regions of the galaxies, especially within the inner 3,000 light-years. Our findings offer a method for astronomers to estimate the gas content using easily obtainable morphological parameters, which is very useful in situations where it is difficult or impossible to obtain direct gas measurements.