Notes. ⁽¹⁾Physical areas encompassing the combined primary beam of the 1.3 and 3 mm mosaics, down to 15%. These areas define the cloud sizes. ⁽²⁾Integrated flux density at 870 μm measured on the ATLASGAL images (Schuller et al. 2009) within the area of the 1.3 mm ALMA images (Col. (2)). ⁽³⁾Cloud mass computed from the 870 μm integrated flux (Col. (4)) assuming and using T_dust = 20 K, 25 K and 30 K for the Young, Intermediate, and Evolved regions (see Col. (8)), respectively. ⁽⁴⁾Flux surface density of the free-free emission at 92.034 GHz, estimated from the integrated flux of the H41α recombination line. Spatial distribution of the ionized gas: HCH II and UCH II consist of <0.05 pc and ~0.1 pc bubbles of ionized gas, respectively; H II are larger regions of ionized gas with a non-spherical structure, some are faint H II regions (see Sect. 4.1 and Motte et al. 2018a). ⁽⁵⁾Classification of the ALMA-IMF protocluster clouds: Young (Y), Intermediate (I), and Evolved (E). Their evolutionary stage is refined from that of Csengeri et al. (2017) by measuring their 1.3 mm to 3 mm flux ratio (Col. (6)) and their estimated free-free emission flux density (Col. (7)). We assume that IR-quiet and IR-bright ATLASGAL clumps are associated with Young and Evolved clouds, respectively. Any evolution of this classification is discussed in Sect. 4.1 and indicated here by an arrow.