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As the precursors to stellar clusters, it is imperative that we understandthe distribution and physical properties of dense molecular gas clouds andclumps. Such a study has been done with the ground-based Bolocam Galactic PlaneSurvey (BGPS). Now the Herschel infrared GALactic plane survey (Hi-GAL) allowsus to do the same with higher quality data and complete coverage of theGalactic plane. We have made a pilot study comparing dense molecular gas clumpsidentified in the Hi-GAL and BGPS surveys, using six $2^\circ \times 2^\circ$regions centered at Galactic longitudes of $\ell = 11^\circ$, 30$^\circ$,41$^\circ$, 50$^\circ$, 202$^\circ$, and $217^\circ$. We adopted the BGPSmethodology for identifying clumps and estimating distances, leading to 6198clumps being identified in our substudy, with 995 of those havingwell-constrained distances. These objects were evenly distributed with Galacticlongitude, a consequence of Hi-GAL being source confusion limited. These clumpsrange in mass from 10$^{-2}$ M$_\odot$ to 10$^{5}$ M$_\odot$, and haveheliocentric distances of up to 16 kpc. When clumps found in both surveys arecompared, we see that distances agree within 1 kpc and ratios of masses are oforder unity. This serves as an external validation for BGPS and instillsconfidence as we move forward to cataloging the clumps from the entirety ofHi-GAL. In addition to the sources that were in common with BGPS, Hi-GAL foundmany additional sources, primarily due to the lack of atmospheric noise. Weexpect Hi-GAL to yield $2\times10^5$ clumps, with 20% having well-constraineddistances, an order of magnitude above what was found in BGPS.

A Galactic Molecular Cloud Clump Catalog from Hi-GAL Data: Method and Initial Results Comparison to BGPS