The gas kinematics are a fundamental tool for understanding the dynamical processes driving the assembly of star clusters and the IMF. Recent and upcoming ALMA-IMF results using N2H+ (1-0) high resolution (~ 4 kau) observations in relatively massive and compact (>~ 1e3 Msun over ~ 1 pc^2) Milky Way protoclusters capture the dense gas kinematics, constraining cluster formation timescales and dynamical processes, such as inflow onto dense star forming "cores". The ALMA-IMF protoclusters discussed here were selected to be relatively simple gas-dominated protoclusters that represent intermediate to evolved hub-filament systems. Despite their apparent simplicity, the kinematic analysis reveals highly dynamic gas and dense core feeding, as well as potential filament rotation in G012. These results lead to the suggestion that processes driving evolution in the gas are ultimately controlling the SFRs and SFEs in these protoclusters. Initial work indicates potentially uncomfortably fast gas consumption timescales (~ 0.3 Myr) in protoclusters G351 and G353; however, gas feeding from the "Mother filaments" may ameliorate this tension to some extent. Newly obtained ALMA data is permitting the evaluation of this hypothesis and preliminary analysis indicates that fast timescales should hold. Broadly, this is in concordance with "fast" scenarios like Global Hierarchical Collapse. The gas kinematics are a critical window for understanding star cluster formation. This analysis provides a useful framework for comparison to both dynamical simulations at high resolution and to far lower resolution extragalactic observations of emerging star clusters, and sets the stage for future observations capable of constraining the early star formation history and conditions in protoclusters.