Young massive stars drive the dynamics of H II regions and their associated neutral and molecular gas through several distinct physical processes. These feedback mechanisms include thermal pressure gradients induced by photoionization and heating, shocks driven by supersonic stellar winds, and three varieties of radiation pressure (EUV continuum, FUV continuum, and the Lyman alpha resonance line). The mechanisms differ in where and how they act on the surrounding material, which, in principle, allows them to be distinguished observationally. Evidence from a variety of regions, from low-luminosity single-star nebulae to the most luminous massive clusters, shows that the relative importance of stellar winds increases with luminosity, as predicted by theory. Recent theoretical advances in the modeling of Lyman alpha transport suggest it may be the dominant feedback mechanism in low-metallicity regions, but direct empirical evidence is still lacking. I present preliminary results from a multi-instrument (MUSE + Local Volume Mapper) study of emission-line kinematics in the giant H II region 30 Doradus in the Large Magellanic Cloud. These results show how the feedback processes evolve from sub-parsec to kiloparsec scales.