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We investigate how the properties of Galactic giant molecular clouds (GMCs)and their denser substructures (clumps) correlate with the local star formationrate. We trace clouds using the $^{12}$CO(3-2) transition, as observed by theCO High Resolution Survey (COHRS). We identify their constituent clumps usingthermal dust emission, as observed by the Herschel infrared GALactic planesurvey (Hi-GAL). We estimate star formation rates in these clouds using 70$\mu$m emission. In total, we match 3,674 clumps to 473 clouds inposition-position-velocity space spanning the Galactic longitude range$10^\circ<\ell<56^\circ$. We find that more massive clouds produce more clumpsand more massive clumps. These clumps have average number densities an order ofmagnitude greater than their host clouds. We find a mean clump mass fraction of$0.20^{+0.13}_{-0.10}$. This mass fraction weakly varies with mass and masssurface density of clouds, and shows no clear dependence on the virialparameter and line width of the clouds. The average clump mass fraction is onlyweakly dependent upon Galactocentric radius. Although the scatter in ourmeasured properties is significant, the star formation rate for clouds isindependent of clump mass fraction. However, there is a positive correlationbetween the depletion times for clouds and clump mass fraction. We find a starformation efficiency per free fall time of $\epsilon_{\mathrm{ff}}=0.15\%$ forGMCs but $\epsilon_{\mathrm{ff}}=0.37\%$ for clumps.

Northern Galactic Molecular Cloud Clumps in Hi-GAL: Clump and Star Formation within Clouds