Stars embedded in active galactic nucleus (Lambda GN) discs or captured by them may scatter onto the supermassive black hole (SMBH), leading to a tidal disruption event (TDE). Using the moving-mesh hydrodynamics simulations with AREPO, we investigate the dependence of debris properties in in-plane TDEs in AGN discs on the disc density and the orientation of stellar orbits relative to the disc gas (pro- and retro-grade). Key findings are: (1) Debris experiences continuous perturbations from the disc gas, which can result in significant and continuous changes in debris energy and angular momentum compared to 'naked' TDEs. (2) Above a critical density of a disc around an SMBH with mass M-center dot[rho(crit) similar to 10(-8) g cm(-3) (M-center dot/10(6) M-circle dot)(-2.5)] for retrograde stars, both bound and unbound debris is fully mixed into the disc. The density threshold for no bound debris return, inhibiting the accretion component of TDEs, is rho(crit, bound) similar to 10(-9) g cm(-3)(M-center dot/10(6) M-circle dot)-2.5. (3) Observationally, AGN-TDEs transition from resembling naked TDEs in the limit of.disc similar to 10-2.crit, bound to fully muffled TDEs with associated inner disc state changes at.discrit, bound, with a superposition of AGN + TDE in between. Stellar or remnant passages themselves can significantly perturb the inner disc. This can lead to an immediate X-ray signature and optically detectable inner disc state changes, potentially contributing to the changing-look AGN phenomenon. (4) Debris mixing can enrich the average disc metallicity over time if the star's metallicity exceeds that of the disc gas. We point out that signatures of AGN-TDEs may be found in large AGN surveys