  This paper combines data from the three preceding papers in order to analyze
the multi-waveband variability and spectral energy distribution of the
Seyfert~1 galaxy NGC~4151 during the December 1993 monitoring campaign. The
source, which was near its peak historical brightness, showed strong,
correlated variability at X-ray, ultraviolet, and optical wavelengths. The
strongest variations were seen in medium energy ($\sim$1.5~keV) X-rays, with a
normalized variability amplitude (NVA) of 24\%. Weaker (NVA = 6\%) variations
(uncorrelated with those at lower energies) were seen at soft $\gamma$-ray
energies of $\sim$100~keV. No significant variability was seen in softer
(0.1--1~keV) X-ray bands. In the ultraviolet/optical regime, the NVA decreased
from 9\% to 1\% as the wavelength increased from 1275~\AA\ to 6900~\AA. These
data do not probe extreme ultraviolet (1200~\AA\ to 0.1~keV) or hard X-ray
(2--50~keV) variability. The phase differences between variations in different
bands were consistent with zero lag, with upper limits of $\ls$0.15~day between
1275~\AA\ and the other ultraviolet bands, $\ls$0.3~day between 1275~\AA\ and
1.5~keV, and $\ls$1~day between 1275~\AA\ and 5125~\AA. These tight limits
represent more than an order of magnitude improvement over those determined in
previous multi-waveband AGN monitoring campaigns. The ultraviolet fluctuation
power spectra showed no evidence for periodicity, but were instead well-fitted
with a very steep, red power-law ($ a = -2.5 $).
  If photons emitted at a ``primary" waveband are absorbed by nearby material
and ``reprocessed" to produce emission at a secondary waveband, causality
arguments require that variations in the secondary band follow those in the
primary band. The tight interband correlation and limits on the ultraviolet and
