Historical reports of pulsed TeV emission from AM Herculis, although later ruled out, led to a search for GeV signatures in magnetically controlled accreting white dwarf binaries using time-resolved analysis techniques with Fermi-LAT data. We present a Fermi-LAT analysis of accretion-driven magnetic systems ({Polars}: CV Hyi, AN UMa, AR UMa, and {IPs}: V515 And, and XY Ari), applying time-resolved (binned likelihood analysis together with TS-gating technique), and temporal analysis to isolate transient gamma-ray signals. Although no persistent emission was detected at the $>$ 5 $\sigma$ level in time-integrated searches, of the above mentioned systems exhibit significant gamma-ray excesses that are spatially coincident with the celestial location of each accretion-driven magnetic system when TS-gated data was considered. The detection of transient, low-level gamma-ray emitters was made possible by the 15-year cadence and sensitivity of the Fermi-LAT. Notably, CV Hyi shows a TS of 203.69 with a weighted significance of $\sigma_w$ = 5.3 $\sigma$, and an orbital modulation at $1.269 \pm 0.004$~hrs, with a detection significance of 5.3 $\sigma$. AN UMa (TS = 237.35; $\sigma_w$ = 5.9 $\sigma$) displays a significant 5.2 $\sigma$ orbital modulation at $1.907 \pm 0.037$~hrs, while AR UMa (TS = 149.95; $\sigma_w$ = 4.6 $\sigma$) reveals a 6.4 $\sigma$ periodic signal at $1.949 \pm 0.055$~hrs distinct from its optical double-peaked profile. Intermediate Polars, V515 And (TS = 227.05; $\sigma_w$ = 5.7 $\sigma$) exhibits pulsed $\gamma$-ray emission at the white dwarf spin period ($465.162 \pm 1.364$~s; 6.7 $\sigma$), and XY Ari (TS = 195.52; $\sigma_w$ = 5.3 $\sigma$) shows modulation at $206.229 \pm 0.115$~s (5.3 $\sigma$). Future studies with more sensitive gamma-ray observatories such as CTA, AMEGO, or e-ASTROGAM, complemented by X-ray and optical monitoring, could provide additional observational data to constrain particle acceleration mechanisms responsible for the emission in these compact binaries.