  We present a study of a luminous, z=0.15, type-2 quasar (log
[L([OIII])/(erg/s)]=42.8) from the Quasar Feedback Survey. It is classified as
'radio-quiet' (log [L(1.4 GHz)/(W/Hz)]=23.8); however, radio imaging reveals ~1
kpc low-power jets (log [Pjet/(erg/s)]=44) inclined into the plane of the
galaxy disk. We combine MUSE and ALMA observations to map stellar kinematics
and ionised and molecular gas properties. The jets are seen to drive
galaxy-wide bi-conical turbulent outflows, reaching W80 = 1000-1300 km/s, in
the ionised phase (traced via optical emission-lines), which also have
increased electron densities compared to the quiescent gas. The turbulent gas
is driven perpendicular to the jet axis and is escaping along the galaxy minor
axis, reaching 7.5 kpc on both sides. Traced via CO(3-2) emission, the
turbulent material in molecular gas phase is one-third as spatially extended
and has 3 times lower velocity-dispersion as compared to ionised gas. The jets
are seen to be strongly interacting with the interstellar medium (ISM) through
enhanced ionised emission and disturbed/depleted molecular gas at the jet
termini. We see further evidence for jet-induced feedback through significantly
higher stellar velocity-dispersion aligned, and co-spatial with, the jet axis
(<5 deg). We discuss possible negative and positive feedback scenarios arising
due to the interaction of the low-power jets with the ISM in the context of
recent jet-ISM interaction simulations, which qualitatively agree with our
observations. We discuss how jet-induced feedback could be an important
feedback mechanism even in bolometrically luminous 'radio-quiet' quasars.
