Recent surveys of dust continuum emission of Galactic star-forming regions have revealed the ubiquity of filamentary structures in molecular clouds. The prevalence of filaments within star-forming regions raises the tantalizing possibility that the star formation efficiency in molecular clouds is strongly dependent on how these dense filaments form and evolve. Using a summary of recent GBT and ALMA results across stellar cluster to protostellar disk scales, I will show how the combined analysis of gas dynamics and chemistry in star-forming regions is critical for testing models of filamentary formation and evolution. I will end by discussing my new Large Program, the Green Bank Ammonia Survey (GAS), that is mapping the dense molecular gas of all the major star-forming molecular clouds within 500 pc. Through GAS, we will connect the gas kinematics and chemistry to the rich, hierarchical cloud structure identified in submillimeter continuum surveys.