To understand the mechanism of star formation it is fundamental to investigate the morphology and kinematics of the gas in clumps and clusters. This requires probing a large homogeneous selection of protoclusters which was recently achieved within the ALMA-IMF Large program. I will present an overview of the ALMA-IMF Large Program which covers a total non-contiguous area of 53 square parsecs towards 15 massive nearby (2 - 5.5 kpc) protoclusters that span a range of well-defined early evolutionary stages and masses (including W51-IRS2, W43). Around 600 compact cores have been extracted from the 1.3mm dust continuum across the 15 protoclusters. Furthermore, ALMA-IMF covers a wealth of molecular lines, such as DCN (3-2), N2D+ (3-2), C18O (2-1), 13CS (5-4), and SiO (5-4). We combine here molecular line and the dust continuum data to explore both the gas and core kinematics with protocluster evolutionary stage, finding a marked difference in the chemistry with evolution.