Context : The determination of the global structure of the planar and extra-planar Milky Way H i disk depends critically on a reliable database but also on reasonable assumptions about the shape of the Milky Way rotation curve .

Aims : We derive the 3-D H i volume density distribution for the Galactic disk out to R \sim 60 kpc .

Methods : Our analysis is based on parameters for the warp and rotation curve derived previously .
The data are taken from the Leiden/Argentine/Bonn all sky 21-cm line survey .

Results : The Milky Way H i disk is significantly warped but shows a coherent structure out to R \sim 35 kpc .
The radial surface density distribution , the densities in the middle of the warped plane , and the H i scale heights all follow exponential relations .
The radial scale length for the surface density distribution of the H i disk is 3.75 kpc .
Gas at the outskirts for 40 \la R \la 60 kpc is described best by a distribution with an exponential radial scale length of 7.5 kpc and a velocity dispersion of 74 km s ^ { -1 } .
Such a highly turbulent medium fits also well with the average shape of the high velocity profile wings observed at high latitudes .
The turbulent pressure gradient of such extra-planar gas is on average in balance with the gravitational forces .
About 10 % of the Milky Way H i gas is in this state .
The large scale H i distribution is lopsided ; for R \ga 15 kpc there is more gas in the south .
The H i flaring indicates that this asymmetry is caused by a dark matter wake , located at R \sim 25 kpc in direction of the Magellanic System .

Conclusions : The H i disk is made up of two major components .
Most prominent is the normal H i disk which can be traced to R \sim 35 kpc .
This is surrounded by a patchy distribution of highly turbulent gas reaching large scale heights but also large radial distances .
At the position of the Sun the exponential scale height in the z direction is 3.9 kpc .
This component resembles the anomalous gas discovered previously in some galaxies .