  We apply a turbulence-regulated model of star formation to calculate the star
formation rate (SFR) of dense star-forming clouds in simulations of jet-ISM
interactions. The method isolates individual clumps and accounts for the impact
of virial parameter and Mach number of the clumps on the star formation
activity. This improves upon other estimates of the SFR in simulations of
jet--ISM interactions, which are often solely based on local gas density,
neglecting the impact of turbulence. We apply this framework to the results of
a suite of jet-ISM interaction simulations to study how the jet regulates the
SFR both globally and on the scale of individual star-forming clouds. We find
that the jet strongly affects the multi-phase ISM in the galaxy, inducing
turbulence and increasing the velocity dispersion within the clouds. This
causes a global reduction in the SFR compared to a simulation without a jet.
The shocks driven into clouds by the jet also compress the gas to higher
densities, resulting in local enhancements of the SFR. However, the velocity
dispersion in such clouds is also comparably high, which results in a lower SFR
than would be observed in galaxies with similar gas mass surface densities and
without powerful radio jets. We thus show that both local negative and positive
jet feedback can occur in a single system during a single jet event, and that
the star-formation rate in the ISM varies in a complicated manner that depends
on the strength of the jet-ISM coupling and the jet break-out time-scale.
