  We observed the high-mass star-forming region G335.579-0.292 with the Atacama
Large Millimeter/submillimeter Array (ALMA) at 226 GHz with an angular
resolution of 0.3'' ($\sim 1000$ au resolution at the source distance).
G335.579-0.292 hosts one of the most massive cores in the Galaxy (G335-MM1).
The continuum emission shows that G335-MM1 fragments into at least five
sources, while molecular line emission is detected in two of the continuum
sources (ALMA1 and ALMA3). We found evidence of large and small scale infall in
ALMA1 revealed by an inverse P-Cygni profile and the presence of a blue-shifted
spot at the center of the first moment map of the CH$_3$CN emission. In
addition, hot gas expansion in the innermost region is unveiled by a
red-shifted spot in the first moment map of HDCO and (CH$_3$)$_2$CO (both with
$E_u > 1100$ K). Our modeling reveals that this expansion motion originates
close to the central source, likely due to reversal of the accretion flow
induced by the expansion of the HII region, while infall and rotation motions
originate in the outer regions. ALMA3 shows clear signs of rotation, with a
rotation axis inclination with respect to the line of sight close to
$90^\circ$, and a system mass (disk + star) in the range of 10-30 M$_\odot$.
