  HS 2325+8205 is a long-period eclipsing dwarf nova with an orbital period
above the period gap (Porb>3 h) and is reported to be a Z Cam-type dwarf nova.
Based on the photometry of the Transiting Exoplanet Survey Satellite (TESS),
the light variation and the quasi-periodic oscillation (QPOs) of HS 2325+8205
are studied. Using Continuous Wavelet Transform (CWT), Lomb-Scargle Periodogram
(LSP), and sine fitting methods, we find for the first time that there is a
QPOs of ~ 2160s in the long outburst top light curves of HS 2325+8205.
Moreover, we find that the oscillation intensity of the QPOs of HS 2325+8205 is
related to the orbital phase, and the intensity in orbital phases 0.5-0.9 are
stronger than in orbital phases 0.1-0.5. Therefore, the relationship between
the oscillation intensity of QPOs and the orbital phase may become a research
window for the origin of QPOs. In addition, we use the LSP to correct the
orbital period of HS 2325+8205 as 0.19433475(6) d.
