Cloud scale molecular gas properties depend on host galaxy and location in the galaxy. PHANGS–ALMA CO(2−1)-based estimates of (left) molecular gas surface density, Σmol, and (right) effective line width, σ v , for three galaxies. All three galaxies are shown at the same physical resolution of 150 pc and using the same logarithmic color stretch. The galaxies show striking differences in their overall surface density and line width, the morphology of their gas distribution at 150 pc scales, and in the distributions of gas and line width within each galaxy. Note that the line width is only measured within pixels detected at high confidence, while the integrated intensity is estimated over an area selected for completeness. See Section 7 for details on the calculation individual maps and Section 8 for similar images of the whole sample.