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We exploit a complete sample of 101\,810 {\it Gaia} DR2 giants, selected inPaper I in the space cylinder with a radius of 700 pc around the Sun and aheight of $|Z|=1800$ pc, using the {\it Gaia} DR2 parallaxes, $G_\mathrm{BP}$and $G_\mathrm{RP}$ photometry, and {\it WISE} $W3$ photometry. We explain thespatial variations of the modes of the observables$G_\mathrm{BP}-G_\mathrm{RP}$ and $G_\mathrm{RP}-W3$ by the spatial variationsof the corresponding reddenings described in the GM20 3D dust distributionmodel. Presented in this paper, GM20 is an advanced version of the modelintroduced by Gontcharov in 2009. GM20 proposes two intersecting dust layers,along the Galactic mid-plane and in the Gould Belt, with exponential verticaland sinusoidal longitudinal variations of the dust spatial density in eachlayer. The Belt layer is an ellipse, oriented nearly between the centre andanticentre of the Galaxy, and with a semi-major and semi-minor axes of 600 and146~pc, respectively. $G_\mathrm{BP}-G_\mathrm{RP}$ and $G_\mathrm{RP}-W3$ givesimilar solutions, but different equatorial layer scale heights of $150\pm15$and $180\pm15$~pc, respectively, and$(G_\mathrm{BP}-G_\mathrm{RP})_0=(1.14\pm0.01)-(0.022\pm0.010)\,|Z|$,$(G_\mathrm{RP}-W3)_0=(1.44\pm0.01)-(0.015\pm0.010)\,|Z|$, where $Z$ is in kpc.We compare GM20 with several 3D reddening models and maps in their ability topredict the observed colour modes. GM20 and the 3D map by Gontcharov appear tobe the best among the models and maps, respectively. However, the most reliablemodels and maps mainly disagree only in their estimates of low reddening,including the reddening across the whole dust layer.

Gaia DR2 giants in the Galactic dust -- II. Application of the reddening maps and models