  We present a detailed study of the molecular gas in the fast AGN-driven
outflow in the nearby radio-loud Seyfert galaxy IC 5063. Using ALMA
observations of a number of tracers (12CO(1-0), 12CO(2-1), 12CO(3-2), 13CO(2-1)
and HCO+(4-3)), we map the differences in excitation, density and temperature
of the gas. The results show that in the immediate vicinity of the radio jet, a
fast outflow, with velocities up to 800 km/s, is occurring of which the gas has
high excitation temperatures in the range 30-55 K, demonstrating the direct
impact of the jet on the ISM. The relative brightness of the CO lines show that
the outflow is optically thin. We estimate the mass of the molecular outflow to
be 1.2 x 10^6 Msol and likely to be a factor 2-3 larger. This is similar to
that of the outflow of atomic gas, but much larger than that of the ionised
outflow, showing that the outflow is dominated by cold gas. The total mass
outflow rate we estimate to be ~12 Msol/yr. The mass of the outflow is much
smaller than the total gas mass of the ISM of IC 5063. Therefore, although the
influence of the radio jet is very significant in the inner regions, globally
speaking the impact will be very modest. We use RADEX modelling to explore the
physical conditions of the molecular gas in the outflow. Models with the
outflowing gas being quite clumpy give the most consistent results and our
preferred solutions have kinetic temperatures in the range 20-100 K and
densities between 10^5 and 10^6 cm^-3. The resulting pressures are 10^6-10^7.5
K cm^-3, about two orders of magnitude higher than in the outer quiescent disk.
The results strongly suggest that the outflow is driven by the radio jet
expanding into a clumpy medium, creating a cocoon of gas which is pushed away
from the jet axis resulting in a lateral outflow, very similar to what is
predicted by numerical simulations.
