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(Abridged) Aims: We aim to use the progressive heating of the gas caused bythe feedback of high-mass young stellar objects (YSOs) to prove the statisticalvalidity of the most common schemes used to define an evolutionary sequence forhigh-mass clumps, and characterise the sensitivity of different tracers to thisprocess. Methods: From the spectroscopic follow-ups of the ATLASGAL TOP100sample, we selected several multiplets of CH3CN, CH3CCH, and CH3OH emissionlines to derive and compare the physical properties of the gas in the clumpsalong the evolutionary sequence. Our findings are compared with resultsobtained from CO isotopologues, dust, and NH3 from previous studies on the samesample. Results: The chemical properties of each species have a major role onthe measured physical properties. Low temperatures are traced by NH3, CH3OH,and CO (in the early phases), the warm and dense envelope can be probed withCH3CN, CH3CCH, and, in evolved sources via CO isotopologues. CH3OH and CH3CNare also abundant in the hot cores, and their high-excitation transitions maybe good tools to study the kinematics in the hot gas surrounding the YSOs thatthese clumps are hosting. All tracers show, to different degrees, progressivewarming with evolution. The relation between gas temperature and L/M isreproduced by a toy model of a spherical, internally heated clump. Conclusions:The evolutionary sequence defined for the clumps is statistically valid and wecould identify the processes dominating in different intervals of L/M. ForL/M<2Lsun/Msun a large quantity of gas is still being accumulated andcompressed at the bottom of the potential well. Between2Lsun/Msun<L/M<40Lsun/Msun the YSOs gain mass and increase in L; the first hotcores appear around L/M=10Lsun/Msun. Finally, for L/M>40Lsun/Msun HII regionsbecome common, showing that dissipation of the parental clump dominates.

ATLASGAL-selected massive clumps in the inner Galaxy: V. Temperature structure and evolution