Schematic evolutionary diagram of subregions in dynamical star-forming clouds, which are qualified as either quiescent or as pre-burst, main burst, or post-burst, determined by following the different phases before, during, and after their main star formation event. Their characteristics, including cloud column density, η-PDF, CMF, and core mass segregation, are illustrated. Top panels: subregions in quiescent or pre-burst regimes present a η-PDF tail close to that found in low-mass star-forming regions and a CMF high-mass end close to the Salpeter slope. Central panels: subregions in their main burst regime harbor an enhanced star formation activity and a strong core mass segregation. They display a η-PDF with a much flatter second tail as well as a top-heavy CMF. Bottom panels: post-burst subregions, under the influence of stellar feedback, have less sustained star formation activity and more complex core mass segregation. They also present a η-PDF with a flat second tail and a CMF that is both top-heavy and bottom-light. The location on the time sequence of the W43-MM2&MM3 subregions are given to summarize the result of the present article.