We examine the physical properties and evolutionary stages of a sample of 17 clumps within 8 Infrared Dark Clouds (IRDCs) by combining existing infrared, millimeter, and radio data with new Bolocam Galactic Plane Survey (BGPS) 1.1 mm data, Very Large Array radio continuum data, and Heinrich Hertz Telescope dense gas (HCO(+) and N(2)H(+)) spectroscopic data. We combine literature studies of star formation tracers and dust temperatures within IRDCs with our search for ultracompact (UC) H II regions to discuss a possible evolutionary sequence for IRDC clumps. In addition, we perform an analysis of mass tracers in IRDCs and find that 8 mu m extinction masses and 1.1 mm BGPS masses are complementary mass tracers in IRDCs except for the most active clumps (notably those containing UC H II regions), for which both mass tracers suffer biases. We find that the measured virial masses in IRDC clumps are uniformly higher than the measured dust continuum masses on the scale of similar to 1 pc. We use (13)CO, HCO(+), and N(2)H(+) to study the molecular gas properties of IRDCs and do not see any evidence of chemical differentiation between hot and cold clumps on the scale of similar to 1 pc. However, both HCO(+) and N(2)H(+) are brighter in active clumps, due to an increase in temperature and/or density. We report the identification of four UC H II regions embedded within IRDC clumps and find that UC H II regions are associated with bright (greater than or similar to 1 Jy) 24 mu m point sources, and that the brightest UC H II regions are associated with "diffuse red clumps" (an extended enhancement at 8 mu m). The broad stages of the discussed evolutionary sequence (from a quiescent clump to an embedded H II region) are supported by literature dust temperature estimates; however, no sequential nature can be inferred between the individual star formation tracers.
