  We disentangle X-ray disk reflection from complex line-of-sight absorption in
the nearby Seyfert NGC 4151, using a suite of Suzaku, NuSTAR, and XMM-Newton
observations. Extending upon earlier published work, we pursue a physically
motivated model using the latest angle-resolved version of the lamp-post
geometry reflection model relxillCp_lp together with a Comptonization
continuum. We use the long-look simultaneous Suzaku/NuSTAR observation to
develop a baseline model wherein we model reflected emission as a combination
of lamp-post components at the heights of 1.2 and 15.0 gravitational radii. We
argue for a vertically extended corona as opposed to two compact and distinct
primary sources. We find two neutral absorbers (one full-covering and one
partial-covering), an ionized absorber ($\log \xi = 2.8$), and a highly-ionized
ultra-fast outflow, which have all been reported previously. All analyzed
spectra are well described by this baseline model. The bulk of the spectral
variability between 1 keV and 6 keV can be accounted for by changes in the
column density of both neutral absorbers, which appear to be degenerate and
inversely correlated with the variable hard continuum component flux. We track
variability in absorption on both short (2 d) and long ($\sim$1 yr) timescales;
the observed evolution is either consistent with changes in the absorber
structure (clumpy absorber at distances ranging from the broad line region
(BLR) to the inner torus or a dusty radiatively driven wind) or a geometrically
stable neutral absorber that becomes increasingly ionized at a rising flux
level. The soft X-rays below 1 keV are dominated by photoionized emission from
extended gas that may act as a warm mirror for the nuclear radiation.
