In recent years, the results of observations of the regions of star formation are more and more evidence in favor of the accretion mechanism for the formation of massive stars. However, the question of the existence of a stellar mass limit remains unclear, above which the accretion mechanism of the disk is insufficient to explain the growth of a high-mass stars. Therefore, it is necessary to study the regions of star formation and associated regions of ionized hydrogen (HII) at the earliest stages of development. Our main science goal is to determine whether rotating hot molecular cores are common around HC HII regions. For that, we mapped using the ALMA in Band 6 the emission arising from two molecules, SO2 and CH3CN, toward several embedded HMYSOs associated with HC HII regions. We analyze the temperature, dynamics, kinematics of rotatinge hot cores. The first-order moment images of molecular lines toward G345.0061+01.794B show a velocity gradient from roughly east to west with average velocities preferentially blueshifted in the West side and redshifted in the East side, and a spot of blueshifted emission towards the peak of the zero-order moment which can be taken as a signature of infall. The best fit is obtained for an infall radius much larger than the beam size, a infinity velocity ??infty, and a central mass of 126.0±8.7??? using the hallmark model of Estalella et al. (2019). Our results indicate that infall motions play a fundamental role in the gas kinematics of this source.