The chemical evolution in high-mass star-forming regions is still poorly constrained .
Studying the evolution of deuterated molecules allows to differentiate between subsequent stages of high-mass star formation regions due to the strong temperature dependence of deuterium isotopic fractionation .
We observed a sample of 59 sources including 19 infrared dark clouds , 20 high-mass protostellar objects , 11 hot molecular cores and 9 ultra-compact H ii regions in the ( 3-2 ) transitions of the four deuterated molecules , DCN , DNC , DCO ^ { + } and N _ { 2 } D ^ { + } as well as their non-deuterated counterpart . The overall detection fraction of DCN , DNC and DCO ^ { + } is high and exceeds 50 % for most of the stages .
N _ { 2 } D ^ { + } was only detected in a few infrared dark clouds and high-mass protostellar objects .
It can be related to problems in the bandpass at the frequency of the transition and to low abundances in the more evolved , warmer stages .
We find median D/H ratios of ~ { } 0.02 for DCN , ~ { } 0.005 for DNC , ~ { } 0.0025 for DCO ^ { + } and ~ { } 0.02 for N _ { 2 } D ^ { + } .
While the D/H ratios of DNC , DCO ^ { + } and N _ { 2 } D ^ { + } decrease with time , DCN/HCN peaks at the hot molecular core stage .
We only found weak correlations of the D/H ratios for N _ { 2 } D ^ { + } with the luminosity of the central source and the FWHM of the line , and no correlation with the H _ { 2 } column density .
In combination with a previously observed set of 14 other molecules ( Paper I ) we fitted the calculated column densities with an elaborate 1D physico-chemical model with time-dependent D-chemistry including ortho- and para-H _ { 2 } states .
Good overall fits to the observed data have been obtained the model .
It is one of the first times that observations and modeling have been combined to derive chemically based best-fit models for the evolution of high-mass star formation including deuteration .