\section{CONCLUSION}
Through our analysis, we showed that the GMAs in the galaxy M100 follow the same basic behaviours as the less massive GMCs in the Milky Way \citep{Solomon_1987} and in the Local Group of galaxies \cite{Fukui_2010}. Such behaviours include both luminous mass and velocity dispersion increasing with cloud radius and the virial mass scaling with the luminous mass of CO, demonstrating that the clouds are virialized. There are clear differences between GMA populations when we separate the galaxy into nuclear, arm and inter-arm regions. Compared to the disk clouds, the nuclear clouds have the highest masses and thus surface densities, and have higher velocity dispersions. From the cumulative mass distributions, our indices were consistent with the expected range of -2.5 to -1.5 \citep{Rosolowsky_2005}, though we saw a steeper index for inter-arm clouds ($\alpha = -2.37$) than for arm clouds ($\alpha = -1.83$), suggesting that the inter-arm population carries more of its mass in lower mass clouds. The agreement of the mean velocity gradients for the arm and inter-arm clouds and the tight correlation of turbulent line width on a one parsec scale with velocity gradient points to turbulent motion dominating over galactic shear motion. The ISM depletion time decreases with increasing cloud surface density and turbulent line width on a one parsec scale, demonstrating that more turbulent clouds form stars more efficiently and denser clouds form stars more efficiently. It is hard to sort out causality, but this is consistent with expectations from turbulence regulated star formation models like \citet{Krumholz_2005}.
