  We present a new approach to tackle the issue of radio loudness in quasars.
We constrain a (simple) prescription for the intrinsic distribution of
radio-to-optical ratios by comparing properties of Monte Carlo simulated
samples with those of observed optically selected quasars. We find strong
evidence for a dependence of the radio luminosity on the optical one, even
though with a large scatter. The dependence of the fraction of radio loud
quasars on apparent and absolute optical magnitudes results in a selection
effect related to the radio and optical limits of current surveys. The
intrinsic distribution of the radio-to-optical ratios shows a peak at
$R^*_{1.4} \sim 0.3$, with only $\simlt 5$ per cent of objects being included
in a high $R^*_{1.4}$ tail which identifies the radio loud regime. No lack or
deficit of sources -- but only a steep transition region -- is present between
the radio loud and radio quiet populations at any $R^*_{1.4}$. We briefly
discuss possible origins for this behaviour (e.g. absence of jets in radio
quiet sources, large range of radiative radio efficiency, different life-times
for the accretion and jet ejection phenomena, ...).
