  We observed Jupiter four times over a full rotation (10 hrs) with the
upgraded Karl G. Jansky Very Large Array (VLA) between December 2013 and
December 2014. Preliminary results at 4-17 GHz were presented in de Pater et
al. (2016); in the present paper we present the full data set at frequencies
between 3 and 37 GHz. Major findings are: (i) the radio-hot belt at
8.5--11$^\circ$N latitude, near the interface between the North Equatorial Belt
(NEB) and the Equatorial Zone (EZ) is prominent at all frequencies (3--37 GHz).
Its location coincides with the southern latitudes of the NEB (7--17$^{\circ}$
N). (ii) Longitude-smeared maps reveal belts and zones at all frequencies at
latitudes $\lesssim |20^\circ|$. The lowest brightness temperature is in the EZ
near a latitude of 4$^\circ$N, and the NEB has the highest brightness
temperature near 11$^\circ$N. The bright part of the NEB increases in
latitudinal extent (spreads towards the north) with deceasing frequency, i.e.,
with depth into the atmosphere. In longitude-resolved maps, several belts, in
particular in the southern hemisphere, are not continuous along the latitude
line, but broken into small segments as if caused by an underlying wave. (iii)
Model fits to longitude-smeared spectra are obtained at each latitude. These
show a high NH$_3$ abundance (volume mixing ratio $\sim 4 \times 10^{-4}$) in
the deep ($P>8-10$ bar) atmosphere, decreasing at higher altitudes due to cloud
formation (e.g., in zones), or dynamics in combination with cloud condensation
(belts). In the NEB ammonia gas is depleted down to at least the 20 bar level
with an abundance of $1.75 \times 10^{-4}$. (iv) Using the entire VLA dataset,
we confirm that the planet is extremely dynamic in the upper layers of the
atmosphere, at $P<$2--3 bar, i.e., at the altitudes where clouds form.
[Abridged]
