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Only 20\% of old field stars have detectable debris discs, leaving open thequestion of what disc, if any, is present around the remaining 80\%. Youngmoving groups allow to probe this population, since discs are expected to havebeen brighter early on. This paper considers the population of F~stars in the23~Myr-old BPMG where we find that 9/12 targets possess discs. We also analysearchival ALMA data to derive radii for 4 of the discs, presenting the firstimage of the 63au radius disc of HD~164249. Comparing the BPMG results to discsamples from $\sim45$~Myr and $\sim150$~Myr-old moving~groups, and to discsfound around field stars, we find the disc incidence rate in youngmoving~groups is comparable to that of the BPMG and significantly higher thanthat of field~stars. The BPMG discs tend to be smaller than those aroundfield~stars. However, this difference is not statistically significant due tothe small number of targets. Yet, by analysing the fractional luminosity vsdisc radius parameter space we find that the fractional luminosities in thepopulations considered drop by two orders of magnitude within the first100~Myr. This is much faster than expected by collisional evolution, implying adecay equivalent to $1/\text{age}^2$. We attribute this depletion to embeddedplanets which would be around 170~$M_\text{earth}$ to cause a depletion on theappropriate timescale. However, we cannot rule out that different birthenvironments of nearby young clusters result in brighter debris discs than theprogenitors of field~stars which likely formed in a more dense environment.

A $~75\%$ Occurrence Rate of Debris Discs around F stars in the $\beta$ Pic Moving Group