  We present a study of molecular gas, traced via CO (3-2) from ALMA data, of
four z< 0.2, `radio quiet', type 2 quasars (log [L(bol)/(erg/s)] = 45.3 - 46.2;
log [L(1.4 GHz)/(W/Hz)] = 23.7 - 24.3). Targets were selected to have extended
radio lobes (>= 10 kpc), and compact, moderate-power jets (1 - 10 kpc; log
[Pjet/(erg/s)]= 43.2 - 43.7). All targets show evidence of central molecular
outflows, or injected turbulence, within the gas disks (traced via
high-velocity wing components in CO emission-line profiles). The inferred
velocities (Vout = 250 - 440 km/s) and spatial scales (0.6 - 1.6 kpc), are
consistent with those of other samples of luminous low-redshift AGN. In two
targets, we observe extended molecular gas structures beyond the central disks,
containing 9 - 53 % of the total molecular gas mass. These structures tend to
be elongated, extending from the core, and wrap-around (or along) the radio
lobes. Their properties are similar to the molecular gas filaments observed
around radio lobes of, mostly `radio loud', Brightest Cluster Galaxies. They
have: projected distances of 5 - 13 kpc; bulk velocities of 100 - 340 km/s;
velocity dispersion of 30 - 130 km/s; inferred mass outflow rates of 4 - 20
Msolar/yr; and estimated kinetic powers of log [Ekin/(erg/s)]= 40.3 - 41.7. Our
observations are consistent with simulations that suggest moderate-power jets
can have a direct (but modest) impact on molecular gas on small scales, through
direct jet-cloud interactions. Then, on larger scales, jet-cocoons can push gas
aside. Both processes could contribute to the long-term regulation of star
formation.
