  We study the multi-phase feedback processes in the central ~3 kpc of the
barred Sy 2 galaxy NGC 5643. We use observations of the cold molecular gas
(ALMA CO(2-1)) and ionized gas (MUSE IFU). We study different regions along the
outflow zone which extends out to ~2.3 kpc in the same direction (east-west) as
the radio jet, as well as nuclear/circumnuclear regions in the host galaxy
disk. The deprojected outflowing velocities of the cold molecular gas (median
Vcentral~189 km s^-1) are generally lower than those of the outflowing ionized
gas, which reach deprojected velocities of up to 750 km s^-1 close to the AGN,
and their spatial profiles follow those of the ionized phase. This suggests
that the outflowing molecular gas in the galaxy disk is being entrained by the
AGN wind. We derive molecular and ionized outflow masses of ~5.2x10^7 Msun and
8.5x10^4 Msun and molecular and ionized outflow mass rates of ~51 Msun yr^-1
and 0.14 Msun yr^-1. Therefore, the molecular phase dominates the outflow mass
and outflow mass rate, while the outflow kinetic power and momentum are similar
in both phases. However, the wind momentum load for the molecular and ionized
outflow phases are ~27-5 and <1, which suggests that the molecular phase is not
momentum conserving while the ionized one most certainly is. The molecular gas
content (~1.5x10^7 Msun) of the eastern spiral arm is approximately 50-70% of
the content of the western one. We interpret this as destruction/clearing of
the molecular gas produced by the AGN wind impacting in the host galaxy. The
increase of the molecular phase momentum implies that part of the kinetic
energy from the AGN wind is transmitted to the molecular outflow. This suggest
that in Sy-like AGN such as NGC 5643, the radiative/quasar and the
kinetic/radio AGN feedback modes coexist and may shape the host galaxies even
at kpc-scales via both positive and (mild) negative feedback.
