Turbulent motions in giant molecular clouds (GMCs) have been observed for decades through the size-linewidth power-law relation. However, the observed scatter of this relation can be large, and questions about the sources of the energy feeding turbulence persist. Simulation results indicate that stellar feedback (processes including radiation pressure and winds) can supply the necessary energy in GMCs. I will present measurements of feedback effects on molecular gas in the Large Magellanic Cloud, the nearest star-forming galaxy to our own. This work uses sub-pc CO and 13CO ALMA maps of nine clouds exhibiting a wide range of star formation activity. I will also describe my plans to investigate the strength of feedback effects on gas measured in a larger range of size scales.
