As the precursors to stellar clusters, it is imperative that we understand the distribution and physical properties of dense molecular gas clouds and clumps. Such a study has been done with the ground-based Bolocam Galactic Plane Survey (BGPS). Now the Herschel infrared GALactic plane survey (Hi-GAL) allows us to do the same with higher quality data and complete coverage of the Galactic plane. Using BGPS methodology for identifying clumps and estimating distances, I compare physical properties of clumps found in both surveys. In addition, I present the beginnings of my work studying HiGAL-identified clumps in the CO High-Resolution Survey (COHRS).