Table~\ref{alpha_table} presents the powerlaw and truncated powerlaw indices, $\alpha$ and $\alpha_\mathrm{trunc}$, respectively; the log of the likelihood ratio, $R$, that the truncated or nontruncated distribution is better, where $R$ being greater than zero means that the data are more consistent with the nontruncated powerlaw and $R$ being smaller than zero means the data are more consistent with the truncated powerlaw; the significance of the result, $p$, where a value close to zero means that the difference between the two distributions is significant; and the truncation mass, $M_\mathrm{trunc}$, defined as the reciprocal of $\lambda$. We see that this truncation mass falls off with radius, as does the number of clouds. \citet{Rosolowsky_2005} showed that for GMCs the powerlaw index, $\alpha$, varies from -2.5 to -1.5. Our results for M100 GMAs fit in this expected range for lower mass systems, but the index for the nuclear population and all of the truncated indices are lower than expected. The mass distribution of the nuclear clouds is very flat, although we note that this population is not well represented by a power law fit because it contains only a small number of $10^8M_{\odot}$ GMAs. We see a clear difference between the distributions of arm and inter-arm populations, where the index for inter-arm is notably quite steep. This implies that most of the mass in the inter-arm region is contained in low-mass clouds, and in high-mass clouds for the arm region \cite{Rosolowsky_2005}.