\section{INTRODUCTION}
Molecular clouds are cold, dense regions of interstellar medium where gravity is able to overcome gas pressure, enabling them to be the sole location of star formation. An improved understanding of the structure of molecular clouds will provide insight into star formation. Here, we catalogue the molecular clouds in the spiral galaxy Messier 100 (M100) of the Virgo cluster to determine whether they follow the behaviours found in previous studies \citep{Solomon_1987} \citep{Fukui_2010}. At masses greater than $10^5 M_{\odot}$, molecular clouds fall into the range of Giant Molecular Clouds (GMCs). However, due to M100's distance of 14.3 Mpc from earth, and the large resolution element of our observations compared to the size of typical GMCs, we are looking at complexes of GMCs called Giant Molecular Associations (GMAs). We determine whether traditional scalings extend to these larger, more massive regions. We also analyze how cloud properties differ between populations within the galaxy. We seek to understand these molecular cloud properties to gain insight into their motion, evolution, and ability to form stars.



