Using Clustering in the Submillimeter to Trace the Evolution of Dusty, Star-forming Galaxies on the Main Sequence With the clear evidence of a main sequence for galaxies in the star formation rate vs. stellar mass plane, it becomes important to understand how galaxies evolve within and along the main sequence with time. Galaxy clustering is a key tool for measuring this evolution: we can measure the dark matter halo mass of classes of galaxies via their observed correlation length, and we know well how dark matter halo masses evolve with time. To date, this tool has been only coarsely applied to the submillimeter-bright, dusty, star-forming galaxy (DSFG) population, recovering the typical halo mass of the Herschel detected galaxies. With the prospect of submillimeter surveys in the next decade covering tens to thousands of square degrees and detecting more typical star-forming galaxies, combined with photometric redshifts from large-area O/IR surveys, clustering measurements will become a precision tool for measuring the evolution of the main sequence in this population.