  We use several main-sequence models to derive distances (and extinctions),
with statistically meaningful uncertainties for 11 star-forming-regions and
young clusters. The model dependency is shown to be small, allowing us to adopt
the distances derived using one model. Using these distances we have revised
the age order for some of the clusters of Mayne et al (2007). The new
(approximate) nominal ages are: 2 Myrs for NGC6530 and the ONC, 3 Myrs for
Lambda Orionis, NGC2264 and Sigma Orionis, 4-5 Myrs for NGC2362, 13 Myrs for h
and chi Per, 20 Myrs for NGC1960 and 40 Myrs for NGC2547. In cases of
significantly variable extinction we have derived individual extinctions using
a revised Q-method (Johnson and Morgan, 1953). These new data show that the
largest remaining uncertainty in deriving an age ordering (and necessarily
ages) is metallicity. We also discuss the use of a feature we term the R-C gap
overlap to provide a diagnostic of isochronal age spreads or varying accretion
histories within a given star-formation-region. Finally, recent derivations of
the distance to the ONC lie in two groups. Our new more precise distance of
391(+12,-9) pc allows us to decisively reject the further distance, we adopt
400 pc as a convenient value.
