The dynamic evolution of star formation leads to the production of a diverse suite of molecules, whose emission reveals great detail about the physical and chemical conditions in which these species form. My collaborators and I use wide-band spectral surveys and mapped observations from the Green Bank Telescope and the IRAM 30-m Telescope to study the large-scale structure within the star-forming regions DR21(OH) and IRAS 20126. We use a multi-component local thermodynamic equilibrium model, CASSIS LTE Python, and a gas-grain chemical model, Nautilus, to determine the environment and formation routes producing this observed emission. With single-dish resolution, the spatial scale we recover links a star-forming core to its parent cloud. Next-generation telescopes, such as the next-generation Very Large Array, will provide high resolution and highly sensitive spectral line surveys of these regions. To prepare for this, we are simulating observations of star-forming regions with the Analytical Protostellar Environment code. We will investigate which physical and environmental factors determine the formation of large organic molecules, and what chemical diversity we can expect to observe with the ngVLA in star-forming systems.