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We aim to estimate if structures, such as cavities, rings, and gaps, arecommon in disks around VLMS and to test models of structure formation in thesedisks. We also aim to compare the radial extent of the gas and dust emission indisks around VLMS, which can give us insight about radial drift. We studied sixdisks around VLMS in the Taurus star-forming region using ALMA Band 7 ($\sim340\,$GHz) at a resolution of $\sim0.1''$. The targets were selected because oftheir high disk dust content in their stellar mass regime. Our observationsresolve the disk dust continuum in all disks. In addition, we detect the$^{12}$CO ($J=3-2$) emission line in all targets and $^{13}$CO ($J=3-2$) infive of the six sources. The angular resolution allows the detection of dustsubstructures in three out of the six disks, which we studied by usingUV-modeling. Central cavities are observed in the disks around stars MHO\,6(M5.0) and CIDA\,1 (M4.5), while we have a tentative detection of amulti-ringed disk around J0433. Single planets of masses$0.1\sim0.4\,M_{\rm{Jup}}$ would be required. The other three disks with noobserved structures are the most compact and faintest in our sample. Theemission of $^{12}$CO and $^{13}$CO is more extended than the dust continuumemission in all disks of our sample. When using the $^{12}$CO emission todetermine the gas disk extension $R_{\rm{gas}}$, the ratio of$R_{\rm{gas}}/R_{\rm{dust}}$ in our sample varies from 2.3 to 6.0, which isconsistent with models of radial drift being very efficient around VLMS in theabsence of substructures. Our observations do not exclude giant planetformation on the substructures observed. A comparison of the size andluminosity of VLMS disks with their counterparts around higher mass stars showsthat they follow a similar relation.