Protoplanetary discs are fundamental to star and planet formation, and their dispersal time-scales critically constrain planet formation models. We present a comprehensive study of disc evolution using a blind survey of 32 young stellar clusters (1-100 Myr, within 500 pc), with membership determined from Gaia data. Our analysis, utilizing 2MASS and WISE infrared data, confirms the expected decrease in disc fraction with stellar age, but reveals a distinct inside-out dispersal signature: the characteristic disc decay time-scale increases significantly with wavelength, from t_short = 1.6±0.1 Myr (1.6 - 4.6 μm) to t_W3 = 4.4±0.3 Myr (12 μm). Critically, we identify a population of long-lived discs, including potential Peter Pan disc candidates, with estimated ages up to ~ 100 Myr, and find that disc dissipation is slower around lower-mass stars (median mass decreases from 0.62 to 0.27 solar mass in clusters older than 40 Myr). Further investigation into 120 of these old disc sources using NEOWISE photometry revealed 23 variable sources, mostly in the 10-20 Myr range, exhibiting irregular variability (Δ(mag) ~ 0.5) that may be linked to structures or planetesimals within the late-stage disc. These results motivate future optical and NIR spectroscopic follow-up to spectroscopically confirm and characterize the physical properties of these remarkably persistent systems.