  We fit various colour-magnitude diagrams (CMDs) of the high-latitude Galactic
globular clusters NGC\,5024 (M53), NGC\,5053, NGC\,5272 (M3), NGC\,5466, and
NGC\,7099 (M30) by isochrones from the Dartmouth Stellar Evolution Database and
Bag of Stellar Tracks and Isochrones for $\alpha$-enrichment
[$\alpha$/Fe]$=+0.4$. For the CMDs, we use data sets from {\it Hubble Space
Telescope}, {\it Gaia}, and other sources utilizing, at least, 25 photometric
filters for each cluster. We obtain the following characteristics with their
statistic uncertainties for NGC\,5024, NGC\,5053, NGC\,5272, NGC\,5466, and
NGC\,7099, respectively: metallicities [Fe/H]$=-1.93\pm0.02$, $-2.08\pm0.03$,
$-1.60\pm0.02$, $-1.95\pm0.02$, and $-2.07\pm0.04$ dex with their systematic
uncertainty 0.1 dex; ages $13.00\pm0.11$, $12.70\pm0.11$, $11.63\pm0.07$,
$12.15\pm0.11$, and $12.80\pm0.17$ Gyr with their systematic uncertainty 0.8
Gyr; distances (systematic uncertainty added) $18.22\pm0.06\pm0.60$,
$16.99\pm0.06\pm0.56$, $10.08\pm0.04\pm0.33$, $15.59\pm0.03\pm0.51$, and
$8.29\pm0.03\pm0.27$ kpc; reddenings $E(B-V)=0.023\pm0.004$, $0.017\pm0.004$,
$0.023\pm0.004$, $0.023\pm0.003$, and $0.045\pm0.002$ mag with their systematic
uncertainty 0.01 mag; extinctions $A_\mathrm{V}=0.08\pm0.01$, $0.06\pm0.01$,
$0.08\pm0.01$, $0.08\pm0.01$, and $0.16\pm0.01$ mag with their systematic
uncertainty 0.03 mag, which suggest the total Galactic extinction
$A_\mathrm{V}=0.08$ across the whole Galactic dust to extragalactic objects at
the North Galactic pole. The horizontal branch morphology difference of these
clusters is explained by their different metallicity, age, mass-loss
efficiency, and loss of low-mass members in the evolution of the core-collapse
cluster NGC\,7099 and loose clusters NGC\,5053 and NGC\,5466.
