Tidal interactions shape the evolution of close-in giant planets, and internal-gravity-wave breaking offers an efficient pathway for dynamical-tide dissipation, though its population-wide impact remains poorly constrained. We aim to quantify wave-breaking tidal dissipation for 550 hot Jupiters, accounting for stellar-parameter uncertainties, and to identify the most promising systems for detecting orbital decay through transit timing. Stellar masses, radii, and ages were homogeneously redetermined from spectroscopic and photometric data using isochrone fitting. For each system, these parameters were propagated through a dedicated MESA model grid to calculate the tidal quality factor, wave-breaking probability, orbital decay rate, and transit- timing diagnostics. Long-term orbital evolution was modelled to predict planetary destruction timescales. Wave breaking is predicted to be largely inactive in pre-intermediate-age main sequence (IAMS) stars. For hosts with masses <1.2M_{sun}_, it becomes effective after the IAMS, while in more massive stars it begins between the IAMS and the terminal-age main sequence (TAMS). The tidal quality factor for systems undergoing wave breaking peaks between 10^6 and 10^7, consistent with population-level inferences. About 43 % of planets, mostly with periods 5-6d. Systems with periods <1d, that could in principle experience the strongest tidal forcing, are unlikely to trigger wave breaking, leaving planets on stable orbits. Conversely, the most rapidly inspiralling systems with high wave-breaking probability may display measurable orbital-period shortening only over multi-decade baselines, eluding immediate detection. By contrast, the demographic imprint of wave breaking on occurrence rates should emerge more readily, with the first signs already visible in current population statistics.

Cone search capability for table J/A+A/709/A60/tablea1 (Spectroscopic and general parameters of the studied systems)