AbstractWe compare the resolved properties of giant molecular clouds (GMCs) in the Small Magellanic Cloud (SMC) and other low mass galaxies to those in more massive spirals. When measured using CO line emission, differences among the various populations of GMCs are fairly small. We contrast this result with the view afforded by dust emission in the Small Magellanic Cloud. Comparing temperature-corrected dust opacity to the distribution of H i suggests extended envelopes of CO-free H₂, implying that CO traces only the highest density H₂ in the SMC. Including this CO-free H₂, the gas depletion time, H₂-to-H i ratio, and H₂-to-stellar mass/light ratio in the SMC are all typical of those found in more massive irregular galaxies.