  We present a detailed analysis of a long, 100 ksec, observation of NGC 4151
by ASCA, contemporaneous with an observation by the CGRO/OSSE. We fit the data
with physical models including an Fe K line and Compton reflection both
relativistically broadened and coupled according to theoretical results. The
model also includes a narrow Fe K component, which is emitted by both an
extended plasma region and the X-ray absorber. Our study of the absorber shows
strong evidence for the presence of more than one partial-covering cloud in the
line of sight. Taking these points into account, our best intrinsic model
includes a Comptonization continuum with an X-ray slope of Gamma=1.9 from a
thermal plasma with an electron kT=70 keV or so and a disk line with an
equivalent width of about 70 eV. The broadening of the line and reflection
indicate their origin from innermost parts of an accretion disk. Our results
indicate that NGC 4151 has an intrinsic X-ray spectrum and variability
properties similar to those of average Seyfert 1s.
