  Tilted disk precession exists in different objects. Negative superhumps
(NSHs) in cataclysmic variable stars (CVs) are hypothesized to arise from the
interaction between the reverse precession of a tilted disk and the streams
from the secondary star. Utilizing TESS photometry, we present a comprehensive
investigation into the tilted disk precession and NSHs in the dwarf nova (DN)
HS 2325+8205, employing eclipse minima, eclipse depths, NSH frequencies, and
NSH amplitudes and the correlation between them as the windows. We report the
discovery of NSHs in HS 2325+8205 with a period of 0.185671(17) d. The NSH
frequency was found to vary with a period of 3.943(9) d, similar to the tilted
disk precession period validated in novae-like star (NL, SDSS J0812) and
intermediate polar (IP, TV Col). The eclipsing minima of O-C were similarly
found to vary cyclically in period 4.135(5) d, showing faster rise than fall.
Furthermore, NSH amplitude varies parabolically, linearly increasing with
periodic variations, potentially linked to changes in disk radius, mass
transfer rate, and apparent area of the hot spot. Additionally, for the first
time in DNe, we observe bi-periodic variations in eclipse depth (P1= 4.131(4) d
and P2= 2.065(2) d ~ Pprec/2), resembling those seen in IPs, suggesting that
variations with P2 are not attributable to the accretion curtain. Moreover, NSH
amplitude and eclipse depth decrease with increasing NSH frequency, while NSH
amplitude correlates positively with eclipse depth.These complex variations
observed across multiple observational windows provide substantial evidence for
understanding of tilted disk precession and NSHs.
