  We present a photometric study of the newly discovered eclipsing IP
$J183221.56-162724.25$ (in short $J1832$) with an orbital period of $8.87hr$.
The system features a box-like deep eclipse with a full width at 50% depth of
$1970\pm2s$ and a large-amplitude coherent pulsation with
$P_\mathrm{obs}\!=\!65.18min$, which represents either the synodic (beat)
period or the spin period of the white dwarf (WD). The period ratio is either
$P_\mathrm{spin}\!/P_\mathrm{orb} = 0.1091$ or $0.1225$, respectively. The
eclipsed light originates almost entirely from the two accretion spots and
columns on the WD, with characteristics indicative of pole flipping. There is
no evidence for an accretion disk, and we identify J1832 as the first deeply
eclipsing stream-fed intermediate polar. Our $grizy$ photometry in eclipse
yielded an $i$-band AB magnitude of the Roche-lobe-filling secondary star of
18.98(3), an extinction $E_\mathrm{B-V}\!=\!0.54\!\pm\!0.17$, and a spectral
type $\sim\,K6$. Dynamic models, fitting the photometry, limit the distance to
between 1270 and 2500pc for masses of the secondary star, $M_2$, between $0.16$
and $1.0M_\mathrm{\odot}$, well within the Gaia EDR3 confidence limits.
Employing a luminosity selection inspired by binary population studies yields a
mean $M_2\!=\!0.32 M_\mathrm{\odot}$ with a 2$\sigma$ upper limit of $0.60
M_\mathrm{\odot}$ and a mean distance d = 1596pc with a 2$\sigma$ upper limit
of 1980pc. The secondary star is located in its Hertzsprung-Russell diagram at
a mean $T_\mathrm{eff,2}\!=\!4120K$ and $log(L_2/L_\mathrm{\odot})\!=\!-0.92$,
from where the binary can evolve into either a polar or an ultracompact binary
with a highly magnetic primary. The system displays a variable accretion rate,
lapses repeatedly into short-lived low states of negligible accretion, and
currently displays an orbital period that decreases on a timescale of
$\tau\!\sim\!3*10^5yr$.

Solar and Stellar Astrophysics;High Energy Astrophysical Phenomena